We should note here that a few features in the red part of the spectrum are not
reproduced. In particular, emissions near 8100, 9000 and 9500 Å are weak or
absent in our synthetic spectra. The emission near 8100 Å may have
contributions from [Fe i], but the relative expected line strengths do not match
the observed profile, and other [Fe i] lines are not seen. Our synthetic
spectrum shows a weak feature, which is caused almost entirely by [Fe ii] lines.
If a weak underlying continuum was removed from the data the discrepancy would
not be as large. Another possibility is poorly known atomic data for these
lines. This may also affect the emission near 9000 Å, which our spectra only
partially reproduce, while we have no suitable candidate for the emission near
9500 Å. The emissions near 9000 and 9500 Å were also seen in SNe 1991bg
and 1999by, while the one near 8100 Å was not [1]}.
